The orbital evolution of asteroids, pebbles and planets from giant branch stellar radiation and winds

Veras, Dimitri; Eggl, Siegfried; Gänsicke, B. T.

doi:10.1093/mnras/stv1047

Cited by 65 publications

(107 citation statements)

References 123 publications

(143 reference statements)

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“…The asteroid further would be too large to be circularized by radiation alone, either through the Yarkovsky effect or Poynting-Robertson drag (Veras et al 2015a(Veras et al , 2015c. One possibility is that some fraction of the asteroid has sublimated.…”

Section: Discussionmentioning

confidence: 99%

High-Speed Photometry of the Disintegrating Planetesimals at Wd1145+017: Evidence for Rapid Dynamical Evolution

Gänsicke

Aungwerojwit

Marsh

et al. 2016

ApJL

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141

146

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We obtained high-speed photometry of the disintegrating planetesimals orbiting the white dwarf WD 1145+017, spanning a period of four weeks. The light curves show a dramatic evolution of the system since the first observations obtained about seven months ago. Multiple transit events are detected in every light curve, which have varying durations (;3-12 minutes) and depths (;10%-60%). The time-averaged extinction is ;11%, much higher than at the time of the Kepler observations. The shortest-duration transits require that the occulting cloud of debris has a few times the size of the white dwarf, longer events are often resolved into the superposition of several individual transits. The transits evolve on timescales of days, both in shape and in depth, with most of them gradually appearing and disappearing over the course of the observing campaign. Several transits can be tracked across multiple nights, all of them recur on periods of ;4.49 hr, indicating multiple planetary debris fragments on nearly identical orbits. Identifying the specific origin of these bodies within this planetary system, and the evolution leading to their current orbits remains a challenging problem.

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Section: Discussionmentioning

confidence: 99%

High-Speed Photometry of the Disintegrating Planetesimals at Wd1145+017: Evidence for Rapid Dynamical Evolution

Gänsicke

Aungwerojwit

Marsh

et al. 2016

ApJL

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141

146

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“…In this case, the exomoon would become an exoring, and this exoring would be subject to a similar type of disruption from close encounters with other planets during gravitational scattering on the WD phase. If the moon survives spin-up, then GB radiation could alter its orbit (Veras, Eggl & Gänsicke 2015a), potentially allowing it to drift closer to the edge of the planet's Hill radius. Just how the orbital parameters of the moon would be affected by this radiation is non-trivial and requires future exploration.…”

Section: Additional Considerationsmentioning

confidence: 99%

“…2 of Mustill et al 2014). By adopting this mass-loss rate, we can derive max(ρ wind ) by assuming a spherically symmetric wind and using equation (5) from Dong et al (2010) or equation (54) from Veras et al (2015a). Consequently, we find max(ρ wind ) = max(Ṁ )/(4πa 2 P v wind ) = 3.1 × 10 −45 ap 30 au −2 M m −3 , assuming that v wind corresponds to the escape speed from a typical WD (4 × 10 3 km s −1 ).…”

Section: A P P E N D I X B : E N C L O S E D M a S S W I T H I N M O mentioning

confidence: 99%

Liberating exomoons in white dwarf planetary systems

Payne¹,

Veras²,

Holman³

et al. 2016

Mon. Not. R. Astron. Soc.

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Previous studies indicate that more than a quarter of all white dwarf (WD) atmospheres are polluted by remnant planetary material, with some WDs being observed to accrete the mass of Pluto in 10 6 yr. The short sinking time-scale for the pollutants indicates that the material must be frequently replenished. Moons may contribute decisively to this pollution process if they are liberated from their parent planets during the post-main-sequence evolution of the planetary systems. Here, we demonstrate that gravitational scattering events amongst planets in WD systems easily trigger moon ejection. Repeated close encounters within tenths of planetary Hill radii are highly destructive to even the most massive, close-in moons. Consequently, scattering increases both the frequency of perturbing agents in WD systems, as well as the available mass of polluting material in those systems, thereby enhancing opportunities for collision and fragmentation and providing more dynamical pathways for smaller bodies to reach the WD. Moreover, during intense scattering, planets themselves have pericentres with respect to the WD of only a fraction of an astronomical unit, causing extreme Hill-sphere contraction, and the liberation of moons into WD-grazing orbits. Many of our results are directly applicable to exomoons orbiting planets around main-sequence stars.

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“…It must also be mentioned that other mechanisms, some of which not yet well understood, could also produce the observed excitation of the MB. One example is the recent work by Veras et al (2015), which models the orbital evolution of asteroids under the effect of stellar radiation and winds. In particular, the authors study the long-lasting Yarkovsky effects on the eccentricity and inclination evolution of the small bodies.…”

Section: Dynamical Excitationmentioning

confidence: 99%

On the current distribution of main belt objects: Constraints for evolutionary models

Michtchenko

Lazzaro

Carvano

2016

A&A

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Context. It is widely accepted that the current distribution of material in the main asteroidal belt (MB) is a product of the evolutionary history of the solar system during its whole lifetime of ∼4.5 billions of years and is, consequently, a major witness of the diverse stages of this evolution. Aims. The purpose of this paper is twofold: first, we study the principal aspects of the distribution of the asteroids in proper element space, mass, and, physical composition for a complete picture of the current MB. Second, we analyze if and how these current distributions can be explained by the long-lasting dynamical effects of the planets on this region of the solar system. Methods. We studied the distribution in the proper element space for the sample that consists of about 350 000 objects whose proper orbital elements are available from the database AstDyS. We studied the distribution in size and physical composition using the most recent and large available datasets. We constructed the dynamical portrait of the MB in form of the dynamical and averaged maps via the spectral analysis method. Results. The main properties of the current distributions of MB objects are identified. A comparison of the distributions of real objects with dynamical maps allows us to detect principal mechanisms of the diffusive transportation of the objects. These mechanisms are related to mean-motion resonances (MMRs) and secular resonances (SRs), overlaying with the slow dissipative Yarkovsky/Yorp drift. Conclusions. We identify the most relevant distributions of the material in the MB and show that many of the current features of the MB can be explained by the interplay of diverse dynamical mechanisms due to the planetary perturbations over 4 Gyr with nongravitational effects, without the need of 'catastrophic' events or 'ad hoc' migration mechanisms during the early stages of the solar system. In this sense, the obtained distributions can provide relevant constraints for modeling the origin and evolution of the MB.

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The orbital evolution of asteroids, pebbles and planets from giant branch stellar radiation and winds

Cited by 65 publications

References 123 publications

High-Speed Photometry of the Disintegrating Planetesimals at Wd1145+017: Evidence for Rapid Dynamical Evolution

High-Speed Photometry of the Disintegrating Planetesimals at Wd1145+017: Evidence for Rapid Dynamical Evolution

Liberating exomoons in white dwarf planetary systems

On the current distribution of main belt objects: Constraints for evolutionary models

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